Milky Way versus Andromeda: a tale of two disks

Yin, Jun; Hou, Jinliang; Prantzos, Nikos; Boissier, S.; Chang, Ruixiang; Shen, Shiyin; Zhang, B.

doi:10.1051/0004-6361/200912316

Cited by 123 publications

(171 citation statements)

References 125 publications

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“…The fact that it is so close makes it not only the ideal candidate for a comparison with similar studies and ongoing surveys taking place with Herschel on our own Galaxy (such as Hi-Gal, Molinari et al 2010), but also the ideal place for studying the interstellar medium of a spiral galaxy. Hinting at some common aspects between the MW and M 31, Yin et al (2009) find very similar gas mass fraction profiles (similar scale lengths but different normalizations) and abundance gradients in the two disks.…”

Section: Introduction An Overall View Of the Interstellar Medium Of Tmentioning

confidence: 76%

TheHerschelExploitation of Local Galaxy Andromeda (HELGA)

Fritz

Gentile

Smith

et al. 2012

A&A

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Context. We have obtained Herschel images at five wavelengths from 100 to 500 μm of a ∼5.5 × 2.5 degree area centred on the local galaxy M 31 (Andromeda), our nearest neighbour spiral galaxy, as part of the Herschel guaranteed time project "HELGA". The main goals of HELGA are to study the characteristics of the extended dust emission, focusing on larger scales than studied in previous observations of Andromeda at an increased spatial resolution, and the obscured star formation. Aims. In this paper we present data reduction and Herschel maps, and provide a description of the far-infrared morphology, comparing it with features seen at other wavelengths. Methods. We used high-resolution maps of the atomic hydrogen, fully covering our fields, to identify dust emission features that can be associated to M 31 with confidence, distinguishing them from emission coming from the foreground Galactic cirrus. Results. Thanks to the very large extension of our maps we detect, for the first time at far-infrared wavelengths, three arc-like structures extending out to ∼21, ∼26 and ∼31 kpc respectively, in the south-western part of M 31. The presence of these features, hosting ∼2.2 × 10 6 M of dust, is safely confirmed by their detection in HI maps. Overall, we estimate a total dust mass of ∼5.8 × 10 7 M , about 78% of which is contained in the two main ring-like structures at 10 and 15 kpc, at an average temperature of 16.5 K. We find that the gas-to-dust ratio declines exponentially as a function of the galacto-centric distance, in agreement with the known metallicity gradient, with values ranging from 66 in the nucleus to ∼275 in the outermost region. Conclusions. Dust in M 31 extends significantly beyond its optical radius (∼21 kpc) and what was previously mapped in the farinfrared. An annular-like segment, located approximately at R 25 , is clearly detected on both sides of the galaxy, and two other similar annular structures are undoubtedly detected on the south-west side even further out.

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Section: Introduction An Overall View Of the Interstellar Medium Of Tmentioning

confidence: 76%

TheHerschelExploitation of Local Galaxy Andromeda (HELGA)

Fritz

Gentile

Smith

et al. 2012

A&A

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“…Based as previously on observational measurements we apply the following rules (Yin et al 2009;Licquia & Newman 2015):…”

Section: Milky Way Sistersmentioning

confidence: 99%

Metal enrichment in a semi-analytical model, fundamental scaling relations, and the case of Milky Way galaxies

Cousin

Buat

Boissier

et al. 2016

A&A

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Context. Gas flows play a fundamental role in galaxy formation and evolution, providing the fuel for the star formation process. These mechanisms leave an imprint in the amount of heavy elements that enrich the interstellar medium. Thus, the analysis of this metallicity signature provides additional constraint on the galaxy formation scenario. Aims. We aim to discriminate between four different galaxy formation models based on two accretion scenarios and two different star formation recipes. We address the impact of a bimodal accretion scenario and a strongly regulated star formation recipe on the metal enrichment process of galaxies. Methods. We present a new extension of the eGalICS model, which allows us to track the metal enrichment process in both stellar populations and in the gas phase. Based on stellar metallicity bins from 0 to 2.5 Z , our new chemodynamical model is applicable for situations ranging from metal-free primordial accretion to very enriched interstellar gas contents. We use this new tool to predict the metallicity evolution of both the stellar populations and gas phase. We compare these predictions with recent observational measurements. We also address the evolution of the gas metallicity with the star formation rate (SFR). We then focus on a subsample of Milky Way-like galaxies. We compare both the cosmic stellar mass assembly and the metal enrichment process of such galaxies with observations and detailed chemical evolution models. Results. Our models, based on a strong star formation regulation, allow us to reproduce well the stellar mass to gas-phase metallicity relation observed in the local Universe. The shape of our average stellar mass to stellar metallicity relations is in good agreement with observations. However, we observe a systematic shift towards high masses. Our M −Z g −SFR relation is in good agreement with recent measurements: our best model predicts a clear dependence with the SFR. Both SFR and metal enrichment histories of our Milky Way-like galaxies are consistent with observational measurements and detailed chemical evolution models. We finally show that Milky Way progenitors start their evolution below the observed main sequence and progressively reach this observed relation at z 0.

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“…The only straightforward conclusion is that YMCs in the age range 50-500 Myr are relatively common in all the most massive star-forming galaxies of the Local Group (M 31, M33, LMC and SMC). The only exception (the Milky Way) may be ascribable to observational biases, but it cannot be excluded that it is instead (at least partly) associated with intrinsic properties of the Milky Way, that appears peculiar under several aspects with respect to the typical spiral galaxies (and to M 31, in particular see Hammer et al 2007;Yin et al 2009). As the samples of M 33 and M 31 should be subject to the same kind of biases (as the distances are similar and the data have been collected with HST in both cases), the difference in the maximum mass limit between the two samples is likely real, and it can probably be ascribed to the difference in total mass between the disks of the two galaxies: larger disks should host more numerous populations of clusters, thus enhancing the probability of producing clusters with higher (maximum) masses (see Gieles 2009, and references therein).…”

Section: The Nature Of M 31 Ymcmentioning

confidence: 99%

An HST/WFPC2 survey of bright young clusters in M 31

Perina

Cohen²,

Barmby

et al. 2010

A&A

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Aims. We present the main results of an imaging survey of possible young massive clusters (YMC) in M 31 performed with the Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope (HST), with the aim of estimating their age and their mass. We obtained shallow (to B ∼ 25) photometry of individual stars in 19 clusters (of the 20 targets of the survey). We present the images and color magnitude diagrams (CMDs) of all of our targets. Methods. Point spread function fitting photometry of individual stars was obtained for all the WFPC2 images of the target clusters, and the completeness of the final samples was estimated using extensive sets of artificial stars experiments. The reddening, age, and metallicity of the clusters were estimated by comparing the observed CMDs and luminosity functions (LFs) with theoretical models. Stellar masses were estimated by comparison with theoretical models in the log(Age) vs. absolute integrated magnitude plane, using ages estimated from our CMDs and integrated J, H, K magnitudes from 2MASS-6X. Results. Nineteen of the twenty surveyed candidates were confirmed to be real star clusters, while one turned out to be a bright star. Three of the clusters were found not to be good YMC candidates from newly available integrated spectroscopy and were in fact found to be old from their CMD. Of the remaining sixteen clusters, fourteen have ages between 25 Myr and 280 Myr, two have older ages than 500 Myr (lower limits). By including ten other YMC with HST photometry from the literature, we assembled a sample of 25 clusters younger than 1 Gyr, with mass ranging from 0.6 × 10 4 M to 6 × 10 4 M , with an average of ∼3 × 10 4 M . Our estimates of ages and masses well agree with recent independent studies based on integrated spectra. Conclusions. The clusters considered here are confirmed to have masses significantly higher than Galactic open clusters (OC) in the same age range. Our analysis indicates that YMCs are relatively common in all the largest star-forming galaxies of the Local Group, while the lack of known YMC older than 20 Myr in the Milky Way may stem from selection effects.

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Milky Way versus Andromeda: a tale of two disks

Cited by 123 publications

References 125 publications

TheHerschelExploitation of Local Galaxy Andromeda (HELGA)

TheHerschelExploitation of Local Galaxy Andromeda (HELGA)

Metal enrichment in a semi-analytical model, fundamental scaling relations, and the case of Milky Way galaxies

An HST/WFPC2 survey of bright young clusters in M 31

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